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On Polar Magnetic Field Reversal in Solar Cycles 21, 22, 23, and 24

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On Polar Magnetic Field Reversal in Solar Cycles 21, 22, 23, and 24 On Polar Magnetic Field Reversal in Solar Cycles 21, 22, 23, and 24 Mykola I. Pishkalo Main Astronomical Observatory, National Academy of Sciences, 27 Zabolotnogo vul., Kyiv, 03680, Ukraine [email protected] Abstract The Sun’s polar magnetic fields change their polarity near the maximum of sunspot activity. We analyzed the polarity reversal epochs in Solar Cycles 21 to 24. There were a triple reversal in the N-hemisphere in Solar Cycle 24 and single reversals in the rest of cases. Epochs of the polarity reversal from measurements of the Wilcox Solar Observatory (WSO) are compared with ones when the reversals were completed in the N- and S-hemispheres. The reversal times were compared with hemispherical sunspot activity and with the Heliospheric Current Sheet (HCS) tilts, too. It was found that reversals occurred at the epoch of the sunspot activity maximum in Cycles 21 and 23, and after the corresponding maxima in Cycles 22 and 24, and one-two years after maximal HCS tilts calculated in WSO. Reversals in Solar Cycles 21, 22, 23, and 24 were completed first in the N-hemisphere and then in the S-hemisphere after 0.6, 1.1, 0.7, and 0.9 years, respectively. The polarity inversion in the near-polar latitude range ±(55–90)˚ occurred from 0.5 to 2.0 years earlier that the times when the reversals were completed in corresponding hemisphere. Using the maximal smoothed WSO polar field as precursor we estimated that amplitude of Solar Cycle 25 will reach 116±12 in values of smoothed monthly sunspot numbers and will be comparable with the current cycle amplitude equaled to 116.4. Keywords Solar cycle, Polar magnetic fields, Polarity reversal, Prediction of solar activity 1. Introduction Studying of evolution of the Sun’s polar magnetic fields is very important for understanding and forecasting of solar activity. Polar fields change their polarity in the epoch of solar maximum and remain predominantly unipolar during the most part of solar cycle. Polar fields are open, and their polarity and distribution determine the global structure of solar corona and the interplanetary magnetic field (see, for example, review by Petrie, 2015, and references therein). There are some difficulties in observation of the polar fields because they are observed from the Earth at large projection angle, and, moreover, the Sun’s northern and southern poles are invisible during some period due to the 7.25˚ inclination of the Earth’s orbit to the plane of the solar equator. To the same, the polar fields are in general significantly weaker than magnetic fields of sunspots and other active features on the middle and low latitudes. Hale (1913) first reported about observed weak general magnetic field of the Sun with opposite polarity in the N- and S-hemispheres. Harold Babcock first observed the asymmetric pattern of the polar reversal. He found that in Solar Cycle 19 the polarity reversal in the S- hemisphere preceded the N-hemisphere by approximately 18 months (Babcock, 1959). The shift in time in the polarity inversion at one pole relative to the other causes an apparent situation when the both poles have the same polarity. It is, of course, only apparent, not real, monopole magnetic situation at the Sun. The evolution of the Sun’s polar magnetic fields is well consistent, in general, with Horace Babcock’s phenomenological model for the solar cycle (Babcock, 1961), with Leighton’s numerical kinematic flux transport model (Leighton, 1969) and, in more details, with advanced modern theories of αΩ-dynamo of the Babcock–Leighton type (see reviews by Charbonneau, 2010; Ossendrijver, 2003; Petrie et al., 2014, and references therein). The polar fields have been actively observed since the 1960s at many observatories. Now they are regularly observed from the ground at the Kitt Peak National Observatory and at the Wilcox Solar Observatory (WSO), and from space using Helioseismic and Magnetic Imager onboard Solar Dynamics Observatory and Solar Optical Telescope onboard the Hinode spacecraft. As a rule, in the N- and S-hemispheres, the polar field changes its polarity non- simultaneously. The asymmetry, or asynchrony, in the reversal process reflects the solar activity asymmetry between the hemispheres (Svalgaard and Kamide, 2013), especially asymmetry of the high-latitudinal magnetic fields (Mordvinov and Yazev, 2014). The reversal of the averaged magnetic field at high latitudes, over ±55˚ latitude, occurs approximately a year earlier than directly at the poles (Pishkalo et al., 2005). Polar field distribution can be studied by indirect methods too, such as distribution of filaments or coronal holes. Filaments (prominences) at high latitudes mark neutral lines between regions with predominantly unipolar and opposite-polarity magnetic flux. Coronal holes, in turn, mark regions with unipolar open magnetic flux. Using the Hα synoptic charts and the data on the polar prominences, Makarov and coauthors (Makarov et al., 1983; Makarov and Sivaraman, 1983; Makarov and Sivaraman, 1986) studied filaments and filament channels distribution at high latitudes in Solar Cycles 11–21 and found epochs of polarity reversals. Moreover, they reported that the reversals repeatedly occur at the poles, i.e. triple reversals were found in the N-hemisphere in Cycles 16, 19, and 20 and in the S- hemisphere in Cycles 12 and 14. In Solar Cycles 21–23 single reversals were identified in both hemispheres according to former results (Durrant and Wilson, 2003; Makarov and Sivaraman, 1986; Pishkalo et al., 2005; Snodgrass et al., 2000; Webb et al., 1984). On the other hand, Mordvinov and Yazev (2014) concluded that a triple reversal occurred at the north in Cycle 21. Many papers are devoted to the polar field reversals in the current Cycle 24. However, the reversal times for Cycle 24 reported by different researchers were different. In particular, Shiota et al. (2012) concluded that the reversal in the N-hemisphere should finish to the middle of 2012. Svalgaard and Kamide (2013) pointed out that, as expected, the reversal first took place in the N- hemisphere. Karna et al. (2014) found that the N-pole changed its polarity in the middle of 2012 and the S-hemisphere will go through reversal at least after 1.5 years later. Upton and Hathaway (2014) forecasted the reversal of the global dipole field of the Sun to be completed by December 2013. Mordvinov and Yazev (2014) found that in Solar Cycle 24 in the N-hemisphere the reversal ended to rotation 2036 (in early 2013). Sun et al. (2015) obtained that, at latitudes over ±60˚, the averaged magnetic field changed its polarity in the N- hemisphere in November 2012 and in the S-hemisphere in March 2014, respectively. Investigation of Pastor Yabar et al. (2015) indicated that the reversals in the N- and S- hemisphere were completed in April 2014 and February 2013, respectively. Pishkalo and Leiko (2016) reported that triple reversal in the N-hemisphere and single reversal in the S-hemisphere were completed to the middle of 2014 (at the beginning of rotation 2150) and in April–May 2015 (at the beginning of rotation 2162), respectively. Gopalswamy et al. (2016) found that the reversal in the S-hemisphere occurred around June 2014 and in the N-hemisphere only by October 2015. Janardhan et al. (2018) found that the reversal in the N-hemisphere was multiple and completed only by November 2014, and in the S-hemisphere it was single and clean reversal, which finished in November 2013. Polar field in the cycle minimum can be considered as a physically-based precursor for solar activity in the maximum of solar cycle (Schatten et al., 1978). There are several predictions of maximal amplitude of Solar Cycle 25, to date, based on the polar field evolution before the cycle minimum (Cameron et al. 2016; Upton and Hathaway, 2018; Wang, 2017). The aim of this work is to compare the time of polarity reversal in the latitude range ±(55– 90)˚ with the time when reversals was finished at the poles, in Solar Cycles 21 to 24, and to estimate the maximal amplitude of the next Cycle 25 using measurements of polar magnetic fields before the cycle minimum as a precursor. 2. Data For the analysis we used monthly and monthly smoothed international sunspot numbers (since 1975) and the corresponding hemispherical values (since 1992) from the Sunspot Index and Long-term Solar Observations (SILSO, http://sidc.oma.be/SISLO, Version 2.0). Hemispherical sunspot numbers from 1975 to 2000, published by Temmer et al. (2002), were also used to analyze period before 1992. Polar magnetic fields measured at the WSO (http://wso.stanford.edu) and the Heliospheric Current Sheet (HCS) tilts calculated by the WSO team in the line-of-sight and radial approaches of the PFSS-model were also analyzed. It should be noted that the polar field strength values, which were determined at the WSO and are used in this paper, are not strength of magnetic field at the poles directly. They represent averaged magnetic fluxes from about the ±55° latitude to the pole for the N- and S-hemisphere. The HCS tilts are maximal latitudes of the magnetic neutral lines at the source surface calculated for each Carrington rotation; they are limited at about ±75° latitude. It should also be mentioned that usually the strength of polar fields are not measured at poles directly. The narrower is the latitude range near the pole where the strength of polar field is measured (or averaged), the closer the time of polarity inversion obtained to the real time when the reversal process is completed in corresponding hemisphere. Epochs of polar magnetic field reversal, i.e. times when the reversal process was completed in each hemisphere, in Solar Cycles 21, 22, and 23 were taken from the paper (Pishkalo et al., 2005), where they were found from analysis of polar prominences and filaments (as a time when polar filaments/prominences disappeared at poles).
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